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Title:
Strongly shocked interstellar gas in IC 443. I - High-resolution molecular observations
Authors:
Wang, Z.; Scoville, N. Z.
Affiliation:
AA(California Institute of Technology, Pasadena), AB(California Institute of Technology, Pasadena)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 386, Feb. 10, 1992, p. 158-169. (ApJ Homepage)
Publication Date:
02/1992
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
INTERSTELLAR GAS, SHOCK WAVE PROPAGATION, SUPERNOVA REMNANTS, ASTRONOMICAL MODELS, CARBON MONOXIDE, EMISSION SPECTRA, MOLECULAR CLOUDS, MOLECULAR GASES, NEAR INFRARED RADIATION
DOI:
10.1086/171001
Bibliographic Code:
1992ApJ...386..158W

Abstract

Interferometric and single-dish observations of the CO (J = 1-0) and (2-1) line emissions are used to investigate the density and velocity structures of shocked interstellar gas in the SNR IC 443. Two adjacent CO emission peaks associated with the brightest 2-micron H2 emission of the area are analyzed. It is proposed that both arise in the same clump of compressed molecular gas; the lower-velocity CO is due to a C-type shock on the front side of the clump where it moves into the ambient molecular cloud exterior to the SNR. The higher-velocity CO is due to a J-shock where outflowing hot gas of the SNR hits the back side of the clump. The clump of gas, accelerated by the ram pressure of the SNR, moves at about 30 km/s with respect to the undisturbed external medium. The model is consistent with both kinematic and morphological evidence indicating that most of the H I gas results from the dissociation of molecules at the J-shock front.

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